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CMB-HD: an Ultra-Deep, High-Resolution Millimeter-Wave Survey Over Half the Sky Response to Astro2020 Decadal Request for Inform

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CMB-HD: an Ultra-Deep, High-Resolution Millimeter-Wave Survey Over Half the Sky Response to Astro2020 Decadal Request for Inform CMB-HD: An Ultra-Deep, High-Resolution Millimeter-Wave Survey Over Half the Sky Response to Astro2020 Decadal Request for Information On behalf of the CMB-HD Collaboration December 9, 2019 Neelima Sehgal1, Simone Aiola2, Yashar Akrami3, Kaustuv Basu4, Mike Boylan-Kolchin5, Sean Bryan6, Caitlin M Casey7,Sebastien´ Clesse8;9, Francis-Yan Cyr-Racine10;11, Luca Di Mascolo12, Simon Dicker13, Thomas Essinger-Hileman14, Simone Ferraro15, George M. Fuller16, Nicholas Galitzki16, Dongwon Han1, Mathew Hasselfield17, Gil Holder18, Bhuvnesh Jain13, Bradley Johnson19, Matthew Johnson20;21, Pamela Klaassen22, Amanda MacInnis1, Mathew Madhavacheril21, Philip Mauskopf6, Daan Meerburg23, Joel Meyers24, Tony Mroczkowski25, Suvodip Mukherjee26, Moritz Munchmeyer21, Sigurd Naess2, Daisuke Nagai27, Toshiya Namikawa28, Laura Newburgh27, Hồ Nam Nguyễn21;29, Michael Niemack30, Benjamin D. Oppenheimer31, Elena Pierpaoli32, Emmanuel Schaan15, Blake Sherwin28, Anzeˇ Slosar33, David Spergel2, Eric Switzer14, Pranjal Trivedi34, Yu-Dai Tsai35, Alexander van 6 2;26 14 arXiv:2002.12714v1 [astro-ph.CO] 28 Feb 2020 Engelen , Benjamin Wandelt , Edward Wollack Executive Summary CMB-HD is a millimeter-wave survey over half the sky, that spans frequencies in the range of 30 to 350 GHz, and is both an order of magnitude deeper and of higher resolution than currently funded surveys. CMB-HD would yield an enormous gain in understanding of both fundamen- tal physics and astrophysics. By providing such a deep, high-resolution millimeter-wave survey (about 0.5 µK-arcmin noise and 15 arcsecond resolution at 150 GHz), CMB-HD will enable major advances. It will allow 1.) the use of gravitational lensing of the primordial microwave background to map the distribution of matter on small scales (k ∼ 10 hMpc−1), which probes both dark mat- ter particle properties and galaxy formation. It will also allow 2.) measurements of the thermal and kinetic Sunyaev-Zel’dovich effects on small scales to map the gas density and gas pressure profiles of halos over a wide field, which probes galaxy evolution and cluster astrophysics. In addition, CMB-HD would allow us to cross critical thresholds in fundamental physics: 3.) ruling out or detecting any new, light (< 0:1 eV), thermal particles, which could potentially be the dark matter, 4.) testing a wide class of multi-field models that could explain an epoch of inflation in the early Universe, and 5.) ruling out a purely primordial origin of galactic magnetic fields. Such a survey would also 6.) monitor the transient sky by mapping the full observing region every few days, which opens a new window on gamma-ray bursts, novae, fast radio bursts, and variable ac- tive galactic nuclei. Moreover, CMB-HD would 7.) provide a census of planets, dwarf planets, and asteroids in the outer Solar System, and 8.) enable the detection of exo-Oort clouds around other solar systems, shedding light on planet formation. Finally, 9.) CMB-HD will provide a catalog of high-redshift dusty star forming galaxies and active galactic nuclei over half the sky down to a flux limit of 0.5 mJy at 150 GHz. The combination of CMB-HD with contemporary ground and space-based experiments will also provide countless powerful synergies. The CMB-HD survey will be made publicly available, with usability and accessibility a priority. CMB-HD aims to deliver this survey in 7.5 years of observing 20,000 square degrees, using two new 30-meter-class off-axis cross-Dragone telescopes to be located at Cerro Toco in the Atacama Desert. Each telescope will field 800,000 detectors (200,000 pixels), for a total of 1.6 million detectors. In terms of technical readiness, the CMB-HD’s detector technology and instrument design have extensive heritage from existing or already funded CMB experiments. Specifically, the technology that has already been demonstrated or is in a mature state are (1) the dichroic, polarization-sensitive TES bolometers at 30/40, 90/150, and 220/280 GHz; (2) the receiver design, and (3) the baseline cross-Dragone telescope design (the latter for a 6-meter dish). These technolo- gies are currently being fielded by the Simons Observatory (SO) [1], which will have first light in 2021, and have also been in development while planning for CMB-S4 [2]. 1 The technology that requires further development are (1) utilizing a laser metrology system to account for thermal effects on the 30-meter dishes, (2) packing the specified detector elements in the receivers, which requires efficient focal plane use, (3) scaling up existing detector and readout production and testing facilities to deliver the specified number of components within a reason- able timeframe, and (4) demonstration of large diameter (> 2 meter) telescope receivers cooled to 100 mK. Some factors mitigating these development risks are that the Green Bank Telescope (GBT) is currently testing a laser metrology system for their 100-meter dish [3]. Recent advances in low-loss silicon [4] could allow a warm first lens resulting in more effective focal plane use [5], and an increase in observation time and/or observing efficiency can compensate for shortfalls in detector count. Moreover, a demonstration of cooling large diameter receivers to 100 mK will be accomplished with the deployment of the SO Large-Aperature Telescope cryostat. In addition, the development of MKID detector technology could substantially reduce the cost of CMB-HD. While the baseline design of CMB-HD employs TES bolometer detectors, if MKID detectors can be robustly demonstrated to achieve comparable sensitivity to TES detectors at millimeter-wavelengths, as some indications suggest may be possible [6], then MKIDs could replace TES detectors resulting in a significant reduction in cost as well as technological com- plexity. The BLAST-TNG, TolTEC, and CCAT-prime projects will soon advance large-format polarization-sensitive MKID arrays [7–9]; TolTEC and CCAT-prime will both deploy arrays at millimeter wavelengths relevant for CMB-HD in the next couple years. Given that a significant amount of required technology is already in a mature state or being deployed in the field in precursor experiments in the next few years, CMB-HD could start this decade. In the first part of the decade, the technology requiring further maturity would need to be developed. Construction of CMB-HD could then ensue in the latter part of the decade. 2 Contents Executive Summary1 1 Science 4 2 Enabling Technology 13 3 Telescope 15 4 Instrumentation 19 5 Facilities 24 6 Operations and Observation Strategy 28 7 Programmatic Issues and Schedule 32 8 Cost 34 References 36 3 1 Science 1. Briefly describe the scientific objectives and the most important measurements required to fulfill these objectives. Feel free to refer to science white papers or references from the literature. 2. Of the objectives, which are the most demanding? Why? 3. Present the highest-level technical requirements (e.g. spatial and spectral resolution, sen- sitivity, timing accuracy) and their relation to the science objectives. 4. For each performance requirement identified, describe as quantitatively as possible the sensitivity of the science objectives to achieve the requirement. If you fail to meet a key requirement, what would be the impact on achieving the science objectives? Two critical advances uniquely enabled by CMB-HD are mapping over half the sky: i) the distribution of all matter on small scales using the gravitational lensing of the cosmic microwave background (CMB), and ii) the distribution of gas density and gas pressure on small scales in and around dark matter halos using the thermal and kinetic Sunyaev-Zel’dovich effects (tSZ and kSZ). The combination of high-resolution and multiple frequency bands in the range of 30 to 350 GHz allows for critical separation of foregrounds from the CMB. That plus the depth of the survey allows one to cross critical thresholds in fundamental physics: i.) ruling out or detecting any new, light, thermal particles, which could potentially be the dark matter, and ii) testing a wide class of multi-field models that could explain an epoch of inflation in the early Universe. CMB-HD would also probe cosmic magnetic fields and open a new window on planetary studies, the transient sky, and the populations of star-forming galaxies and active galactic nuclei. A summary of the primary science questions motivating the CMB-HD survey are given below and discussed in more detail in the accompanying science white paper and CMB-HD APC [10, 11]. • What is the distribution of matter on small scales? • What are the particle properties of dark matter? • How did gas evolve in and around dark matter halos? • How did galaxies form? • Do new light particles exist that were in equilibrium with known particles in the early Universe? • Do axion-like particles exist? • Do primordial gravitational waves exist from an epoch of inflation? 4 • If inflation happened, did it arise from multiple or a single new field? • What is the census of bodies in the outer Solar System? • Do Oort clouds exist around other stars? • What is the physics behind the various bright transient phenomena in the sky? • What are the population distributions of star-forming galaxies and active galactic nuclei? • Was the early Universe magnetized and did that provide the seeds of galactic magnetic fields? 1.1 Science Objectives To answer the science questions listed above, CMB-HD has the following science objectives: 1. Measure the small-scale matter power spectrum from weak gravitational lensing using the CMB as a backlight; with this CMB-HD aims to distinguish between a matter power spectrum predicted by models that can explain observational puzzles of small-scale structure, and that predicted by vanilla cold dark matter (CDM), with a significance of at least 8σ. This measure- ment would be a clean measurement of the matter power spectrum on these scales, free of the use of baryonic tracers.
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